银河系ISM中硅的X射线吸收：气体成分
Silicon X-ray absorption in the Galactic ISM: the gaseous component
摘要：
我们提出了一个详细的分析的气体成分的Si K边缘使用高分辨率的钱德拉光谱的低质量X射线二进制文件。我们用修正的ISMab模型拟合光谱，包括所有Si离子物种的新的光吸收截面计算。我们估计列密度Si i，Si ii，Si iii，Si xii和Si xiii，跟踪温暖，中间温度和热阶段的银河系星际介质。我们发现，前两相的离子分数是相似的。这可能是由于由温度决定的等离子体的物理状态，或者由于在源附近存在吸收剂材料。我们的研究结果强调了在试图解决固体成分之前，需要对气体成分进行准确建模。
英文摘要：
We present a detailed analysis of the gaseous component of the Si K edge using high-resolution Chandra spectra of low-mass X-ray binaries. We fit the spectra with amodified version of the ISMabs model, including new photoabsorption cross sectionscomputed for all Si ionic species. We estimate column densities for Si i, Si ii, Si iii, Si xii and Si xiii, which trace the warm, intermediate temperature and hot phases of the Galactic interstellar medium. We find that the ionic fractions of the first two phases are similar. This may be due to the physical state of the plasma determined by the temperature or to the presence of absorber material in the close vicinity of the sources. Our findings highlight the need for accurate modeling of the gaseous component before attempting to address the solid component.
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